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Argyre Planitia

Argyre Planitia[2] /ˈɑːrdʒəriː/ is a plain located within the impact basin Argyre[a] in the southern highlands of Mars. Its name comes from a map produced by Giovanni Schiaparelli in 1877; it refers to Argyre, a mythical island of silver in Greek mythology.

Argyre Planitia
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Colorized topographic map of Argyre basin and its surroundings, from the MOLA instrument of Mars Global Surveyor.
LocationArgyre quadrangle, Mars
Coordinates49°42′S 316°00′E / 49.7°S 316.0°E / -49.7; 316.0
Diameter1,700 km (1,100 mi)[1]
Depth5.2 km (17,000 ft)
EponymLegendary island Argyre

Argyre is centered at 49°42′S 316°00′E / 49.7°S 316.0°E / -49.7; 316.0 and lies between 35° and 61° S and 27° and 62° W in the Argyre quadrangle. The basin is approximately 1,700 km (1,100 mi) wide[1] and drops 5.2 km (17,000 ft) below the surrounding plains; it is the second-deepest impact basin on Mars after Hellas. The crater Galle, located on the east rim of Argyre at 51°S 31°W / 51°S 31°W / -51; -31, strongly resembles a smiley face.

The basin was formed by a giant impact event by an impactor around 200 kilometres (120 mi) in diameter during the Late Heavy Bombardment of the early Solar System, approximately 4-3.8 billion years ago,[4][5] and may be one of the best preserved ancient impact basins from that period. Argyre is surrounded by rugged massifs which form concentric and radial patterns around the basin. Several mountain ranges are present, some of these mountain ranges include Charitum and Nereidum Montes.[6]

Past water flows

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Four large Noachian epoch channels lie radial to the basin. Three of these channels (Surius Vallis, Dzígai Vallis, and Pallacopas Vallis) flowed into Argyre from the south and east through the rim mountains. The fourth, Uzboi Vallis, appears to have flowed out from the basin's north rim to the Chryse region and may have drained a lake of melting ice within the basin. A smaller outflow channel named Nia Valles is relatively fresh-looking, and probably formed during the early Amazonian after the major fluvial and lacustrine episodes had finished.[7]

The original basin floor is buried with friable, partially deflated layered material that may be lake sediment. No inner rings are visible; however, isolated massifs within the basin may be remnants of an inner ring.[6]

Past habitability

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After the formation of the impact basin, heat from the impact event along with geothermal heating may have allowed for liquid water to persist for many millions of years. The lake's volume could have been equal to that of Earth's Mediterranean Sea. The basin would have supported a regional environment favorable for the origin and the persistence of life.[8] This region shows a great deal of evidence of glacial activity with flow features, crevasse-like fractures, drumlins, eskers, tarns, arêtes, cirques, horns, U-shaped valleys, and terraces. Because of the shapes of Argyre sinuous ridges, the authors agree with previous publications in which they are eskers.[9]

Based on morphometrical and geomorphological analysis of the Argyre eskers and their immediate surroundings, it was suggested that they formed beneath an approximately 2 km thick, stagnant (i.e., stationary) ice sheet around 3.6 billion years ago. This stagnant body of ice might have resembled a Piedmont-style glacier comparable to today's Malaspina Glacier in Alaska.[10]

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  • The southern rim of Argyre basin, formed by the Charitum Montes. Adjacent are sinuous ridges, theorized to be glacial eskers. The crater Galle is seen in the background. 
    The southern rim of Argyre basin, formed by the Charitum Montes. Adjacent are sinuous ridges, theorized to be glacial eskers. The crater Galle is seen in the background.
  • MOLA maps showing the geographic context of Argyre. 
    MOLA maps showing the geographic context of Argyre.
  • MOLA map showing boundaries for Argyre Planitia and other regions 
    MOLA map showing boundaries for Argyre Planitia and other regions
  • Gullies south of Argyre appear to be unequivocal evidence of water erosion. 
    Gullies south of Argyre appear to be unequivocal evidence of water erosion.
  • Scene in Argyre quadrangle with gullies, alluvival fans, and hollows, as seen by HiRISE under HiWish program. Enlargements of parts of this image are below. 
    Scene in Argyre quadrangle with gullies, alluvival fans, and hollows, as seen by HiRISE under HiWish program. Enlargements of parts of this image are below.
  • Several levels of alluvial fans, as seen by HiRISE under HiWish program. Locations of these fans are indicated in the previous image. 
    Several levels of alluvial fans, as seen by HiRISE under HiWish program. Locations of these fans are indicated in the previous image.
  • Small, well-formed alluvial fan, as seen by HiRISE under HiWish program. Location of this fan is shown in an image displayed above. 
    Small, well-formed alluvial fan, as seen by HiRISE under HiWish program. Location of this fan is shown in an image displayed above.
  • Enlargement of above image showing hollows with box showing the size of a football field, as seen by HiRISE under HiWish program. 
    Enlargement of above image showing hollows with box showing the size of a football field, as seen by HiRISE under HiWish program.
  • Gullies, as seen by HiRISE under HiWish program. Location is Nereidum Montes. 
    Gullies, as seen by HiRISE under HiWish program. Location is Nereidum Montes.
  • Surface in Argyre quadrangle as seen by HiRISE, under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long. 
    Surface in Argyre quadrangle as seen by HiRISE, under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.
  • CTX image showing context for the next image. A group of channels are visible in this image. 
    CTX image showing context for the next image. A group of channels are visible in this image.
  • Close-up of surface in Argyre quadrangle, as seen by HiRISE, under the HiWish program. 
    Close-up of surface in Argyre quadrangle, as seen by HiRISE, under the HiWish program.

Interactive Mars map

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Map of Mars Acheron FossaeAcidalia PlanitiaAlba MonsAmazonis PlanitiaAonia PlanitiaArabia TerraArcadia PlanitiaArgentea PlanumArgyre PlanitiaChryse PlanitiaClaritas FossaeCydonia MensaeDaedalia PlanumElysium MonsElysium PlanitiaGale craterHadriaca PateraHellas MontesHellas PlanitiaHesperia PlanumHolden craterIcaria PlanumIsidis PlanitiaJezero craterLomonosov craterLucus PlanumLycus SulciLyot craterLunae PlanumMalea PlanumMaraldi craterMareotis FossaeMareotis TempeMargaritifer TerraMie craterMilankovič craterNepenthes MensaeNereidum MontesNilosyrtis MensaeNoachis TerraOlympica FossaeOlympus MonsPlanum AustralePromethei TerraProtonilus MensaeSirenumSisyphi PlanumSolis PlanumSyria PlanumTantalus FossaeTempe TerraTerra CimmeriaTerra SabaeaTerra SirenumTharsis MontesTractus CatenaTyrrhena TerraUlysses PateraUranius PateraUtopia PlanitiaValles MarinerisVastitas BorealisXanthe Terra
The image above contains clickable links Interactive image map of the global topography of Mars. Hover over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.


See also

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Notes

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  1. ^ Officially, Argyre is an albedo feature.[3]

References

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  1. ^ a b Hiesinger, Harald; Head III, James W. (August 2002). "Topography and morphology of the Argyre Basin, Mars: implications for its geologic and hydrologic history". Planetary and Space Science. 50 (10–11): 939–981. Bibcode:2002P&SS...50..939H. doi:10.1016/S0032-0633(02)00054-5.
  2. ^ "Argyre Planitia". Gazetteer of Planetary Nomenclature. USGS Astrogeology Science Center. Retrieved 29 November 2013.
  3. ^ "Argyre". Gazetteer of Planetary Nomenclature. USGS Astrogeology Science Center. Retrieved 29 November 2013.
  4. ^ Branco, Hely C.; Miljkovic, Katarina; Plesa, Ana‐Catalina (April 2024). "New Numerically Derived Scaling Relationships for Impact Basins on Mars". Journal of Geophysical Research: Planets. 129 (4). doi:10.1029/2023JE008217. ISSN 2169-9097.
  5. ^ Bottke, William F.; Norman, Marc D. (30 August 2017). "The Late Heavy Bombardment". Annual Review of Earth and Planetary Sciences. 45 (1): 619–647. doi:10.1146/annurev-earth-063016-020131. ISSN 0084-6597.
  6. ^ a b 'Topography and morphology of the Argyre Basin, Mars Archived 2021-02-04 at the Wayback Machine.' Hiesinger & Head.
  7. ^ Argyre Planitia and the Mars Global Hydrologic Cycle'. Parker et al.
  8. ^ Fairén Alberto G.; Dohm James M.; Rodríguez J. Alexis P.; Uceda Esther R.; Kargel Jeffrey; Soare Richard; Cleaves H. James; Oehler Dorothy; Schulze-Makuch Dirk; Essefi Elhoucine; Banks Maria E.; Komatsu Goro; Fink Wolfgang; Robbins Stuart; Yan Jianguo; Miyamoto Hideaki; Maruyama Shigenori & Baker Victor R. (February 2016). "The Argyre Region as a Prime Target for in situ Astrobiological Exploration of Mars" (PDF). Astrobiology. 16 (2): 143–158. Bibcode:2016AsBio..16..143F. doi:10.1089/ast.2015.1396. PMID 26836592. Retrieved 12 March 2016.
  9. ^ Dohm, J.; Hare, T.; Robbins, S.; Williams, J.-P.; Soare, R.; El-Maarry, M.; Conway, S.; Buczkowski, D.; Kargel, J.; Banks, M.; Fairén, A.; Schulze-Makuch, D.; Komatsu, G.; Miyamoto, H.; Anderson, R.; Davila, A.; Mahaney, W.; Fink, W.; Cleaves, H.; Yan, J.; Hynek, B.; Maruyama, S. (2015). "Geological and hydrological histories of the Argyre province, Mars" (PDF). Icarus. 253: 66–98. Bibcode:2015Icar..253...66D. doi:10.1016/j.icarus.2015.02.017.
  10. ^ Bernhardt, H.; Hiesinger, H.; Reiss, D.; Ivanov, M. A.; Erkeling, G. (2013). "Putative eskers and new insights into glacio-fluvial depositional settings in southern Argyre Planitia, Mars". Planetary and Space Science Conference. 85: 261–278. Bibcode:2013P&SS...85..261B. doi:10.1016/j.pss.2013.06.022.
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